As mentioned above, theoretical predictions give \(1.5 \le \gamma \le 2.5\)  [1]}, [2]}, [3]}, [4]}. If the effects of baryons or stellar heating are important, the spike index might be close to the smallest extreme value \(\gamma =1.5\)  [1]}, [2]}, [3]}. In fact, this stellar heating effect is due to the dynamical friction between stars and dark matter. Therefore, in a BH-LMXB, the continuous gravitational scattering between the companion star and dark matter might provide the similar stellar heating effect to reduce the spike index to a smaller value. Nevertheless, the case for BH-LMXB is somewhat different from the stellar heating scenario discussed in [1]}, [2]}. There is only one companion object in a BH-LMXB while many stars are involved in the stellar heating scenario. However, recent simulations show that the dynamical friction of the companion object with a large mass ratio \(q\)  would increase the kinetic energy of the dark matter particles in the halo and somewhat decrease the dark matter density [10]}, which apparently reduces the spike index. Although this is not identical to the stellar heating scenario, both processes involve the dynamical friction to re-distribute the dark matter density.
